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The star-forming history of the young cluster NGC 2264UBVRI H-alpha photographic photometry was obtained for a sample of low-mass stars in the young open cluster NGC 2264 in order to investigate the star-forming history of this region. A theoretical H-R diagram was constructed for the sample of probable cluster members. Isochrones and evolutionary tracks were adopted from Cohen and Kuhi (1979). Evidence for a significant age spread in the cluster was found amounting to over ten million yr. In addition, the derived star formation rate as a function of stellar mass suggests that the principal star-forming mass range in NGC 2264 has proceeded sequentially in time from the lowest to the highest masses. The low-mass cluster stars were the first cluster members to form in significant numbers, although their present birth rate is much lower now than it was about ten million yr ago. The star-formation rate has risen to a peak at successively higher masses and then declined.
Document ID
19840033461
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Adams, M. T.
(Kitt Peak National Observatory; Steward Observatory Tucson, AZ, United States)
Strom, K. M.
(Kitt Peak National Observatory Tucson, AZ, United States)
Strom, S. E.
(Kitt Peak National Observatory Tucson, AZ, United States)
Date Acquired
August 12, 2013
Publication Date
December 1, 1983
Publication Information
Publication: Astrophysical Journal Supplement Series
Volume: 53
ISSN: 0067-0049
Subject Category
Astrophysics
Accession Number
84A16248
Funding Number(s)
CONTRACT_GRANT: NASA ORDER A-88923-B
Distribution Limits
Public
Copyright
Other

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